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In a two component advective flow around a compact object, a high viscosityKeplerian disk is flanked by a low angular momentum and low viscosity flowwhich forms a centrifugal pressure supported shock wave close to the blackhole. The post-shock region which behaves as a Compton cloud becomesprogressively smaller during the outburst as the spectra change from the hardstate to the soft state in order to satisfy Rankine-Hugoniot relation inpresence of cooling. The resonance oscillation of the shock wave which causeslow frequency quasi-periodic oscillations (QPOs) also allows us to obtain theshock location from each observed QPO frequency. Applying the theory oftransonic flow with Compton cooling and viscosity, we obtain the viscosityparameter $\alpha_{SK}$ required for the shock to form at those places in thelow-Keplerian component. When we compare the evolution of $\alpha_{SK}$ foreach outburst, we arrive at a major conclusion: In each source, the advectiveflow component typically requires exactly a similar value of $\alpha_{SK}$ whentransiting from one spectral state to another (e.g., from hard state to softstate through intermediate states and the other way around in the decliningphase). Most importantly, these $\alpha_{SK}$ values in the low-angularmomentum advective component are fully self-consistent in the sense that theyremain below critical value $\alpha_{cr}$ required to form a Keplerian disk.For a further consistency check, we compute the $\alpha_K$ of the Kepleriancomponent, and find that in each of the objects, $\alpha_{SK}$ $<$$\alpha_{cr}$ $<$ $\alpha_K$.

Possible range of viscosity parameter to trigger black hole candidates to exhibit different states of outbursts